Figure 18 from NULLING DATA REDUCTION AND ON-SKY PERFORMANCE OF THE LARGE BINOCULAR TELESCOPE INTERFEROMETER

Image Details

View Article Bookmark & Share

Choose export citation format:

Export Citation

Hi-Resolution Export to PDF PPT Format

NULLING DATA REDUCTION AND ON-SKY PERFORMANCE OF THE LARGE BINOCULAR TELESCOPE INTERFEROMETER

Authors: D. Defrère, P. M. Hinz, B. Mennesson, W. F. Hoffmann, R. Millan-Gabet, A. J. Skemer, V. Bailey, W. C. Danchi, E. C. Downey, O. Durney, P. Grenz, J. M. Hill, T. J. McMahon, M. Montoya, E. Spalding, A. Vaz, O. Absil, P. Arbo, H. Bailey, G. Brusa, G. Bryden, S. Esposito, A. Gaspar, C. A. Haniff, G. M. Kennedy, J. M. Leisenring, L. Marion, M. Nowak, E. Pinna, K. Powell, A. Puglisi, G. Rieke, A. Roberge, E. Serabyn, R. Sosa, K. Stapeldfeldt, K. Su, A. J. Weinberger, and M. C. Wyatt

2016 The Astrophysical Journal 824 66.

Provider: AAS Journals

Caption: Figure 18.

Relative error on the flux estimate as function of the inner and outer radii of the background annulus used for aperture photometry. The resulting error on the source null can simply be obtained by multiplying these values by the null depth. For instance, for a thin annulus located at ∼1.7λ/D (i.e., the position of the first Airy ring) and a typical null depth of 1%, the error on the source null amounts to ∼0.02%. In practice, the position of the background annulus is chosen so that the resulting error on the source null is smaller than 0.01%.

Other Images in This Article

Copyright and Terms & Conditions